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In the framework of studies of the CMB polarization and its Galacticforegrounds, the angular power spectra of thermal dust polarization maps haverevealed an intriguing E/B asymmetry and a positive TE correlation. Ininterpretation studies of these observations, magnetized ISM dust clouds havebeen treated as filamentary structures only; however, sheet-like shapes arealso supported by observational and theoretical evidence. In this work, westudy the influence of cloud shape and its connection to the local magneticfield on angular power spectra of thermal dust polarization maps. We simulaterealistic filament-like and sheet-like interstellar clouds, and generatesynthetic maps of their thermal dust polarized emission using the software$Asterion$. We compute their polarization power spectra in multipole range$\ell \in [100,500]$ and quantify the E/B power asymmetry through the $R_{EB}$ratio, and the correlation coefficient $r^{TE}$ between T and E modes. Wequantify the dependence of $R_{EB}$ and $r^{TE}$ values on the offset angle(between longest cloud axis and magnetic field) and inclination angle (betweenline-of-sight and magnetic field) for both cloud shapes embedded either in aregular or a turbulent magnetic field. We find that both cloud shapes cover thesame regions of the ($R_{EB}$, $r^{TE}$) parameter space. The dependence oninclination and offset angles are similar for both shapes although sheet-likestructures generally show larger scatter. In addition to the known dependenceon the offset angle, we find a strong dependence of $R_{EB}$ and $r^{TE}$ onthe inclination angle. The fact that filament-like and sheet-like structuresmay lead to polarization power spectra with similar ($R_{EB}$, $r^{TE}$) valuescomplicates their interpretation. In future analyses, this degeneracy should beaccounted for as well as the connection to the magnetic field geometry.

Polarization power spectra and dust cloud morphology